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Valles Marineris cloud trails
Distinctive cloud trails are identified in Mars Reconnaissance Orbiter Mars Color Imager (MARCI) images over specific locations associated with Valles Marineris and Noctis Labyrinthus and at perihelion solar longitudes (LS = 230°–260°). High‐contrast surface shadows are well defined, as cast from th...
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Published in: | Journal of Geophysical Research. B. Solid Earth 2009-11, Vol.114 (E11), p.n/a |
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creator | Clancy, R. Todd Wolff, Michael J. Cantor, Bruce A. Malin, Michael C. Michaels, Timothy I. |
description | Distinctive cloud trails are identified in Mars Reconnaissance Orbiter Mars Color Imager (MARCI) images over specific locations associated with Valles Marineris and Noctis Labyrinthus and at perihelion solar longitudes (LS = 230°–260°). High‐contrast surface shadows are well defined, as cast from their eastern margins, supporting altitude and optical depth determinations. These relatively high altitude clouds (40–50 km) exhibit narrow latitudinal widths (25–75 km) in comparison to extended longitudinal dimensions (400–1000 km). MARCI multispectral imaging of cloud surface shadows in five wavelength channels (260, 320, 437, 546, and 653 nm) yields the wavelength dependence of cloud extinction optical depth, revealing a range of small cloud particle sizes (reff = 0.2–0.5 μm) and moderate cloud optical depths (0.03–0.10 visible and 0.1–0.2 ultraviolet). Local time and temporal sampling characteristics of MARCI cloud images indicate that these clouds develop very rapidly in afternoon hours (1300–1500 LT), reach their full longitudinal extents within |
doi_str_mv | 10.1029/2008JE003323 |
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Todd ; Wolff, Michael J. ; Cantor, Bruce A. ; Malin, Michael C. ; Michaels, Timothy I.</creator><creatorcontrib>Clancy, R. Todd ; Wolff, Michael J. ; Cantor, Bruce A. ; Malin, Michael C. ; Michaels, Timothy I.</creatorcontrib><description>Distinctive cloud trails are identified in Mars Reconnaissance Orbiter Mars Color Imager (MARCI) images over specific locations associated with Valles Marineris and Noctis Labyrinthus and at perihelion solar longitudes (LS = 230°–260°). High‐contrast surface shadows are well defined, as cast from their eastern margins, supporting altitude and optical depth determinations. These relatively high altitude clouds (40–50 km) exhibit narrow latitudinal widths (25–75 km) in comparison to extended longitudinal dimensions (400–1000 km). MARCI multispectral imaging of cloud surface shadows in five wavelength channels (260, 320, 437, 546, and 653 nm) yields the wavelength dependence of cloud extinction optical depth, revealing a range of small cloud particle sizes (reff = 0.2–0.5 μm) and moderate cloud optical depths (0.03–0.10 visible and 0.1–0.2 ultraviolet). Local time and temporal sampling characteristics of MARCI cloud images indicate that these clouds develop very rapidly in afternoon hours (1300–1500 LT), reach their full longitudinal extents within <2 h time scales, and often reoccur on successive afternoons. Mars Global Surveyor Mars Orbital Camera imaging in previous Mars years indicates these clouds are annually repeating. These observed characteristics suggest a cloud formation mechanism that is specific to ∼50 km horizontal and vertical scales, transports water vapor and dust upward from lower levels, exists during the afternoon, and is likely associated with the mesoscale atmospheric circulations induced by the near‐equatorial canyons of Mars. 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Todd</creatorcontrib><creatorcontrib>Wolff, Michael J.</creatorcontrib><creatorcontrib>Cantor, Bruce A.</creatorcontrib><creatorcontrib>Malin, Michael C.</creatorcontrib><creatorcontrib>Michaels, Timothy I.</creatorcontrib><title>Valles Marineris cloud trails</title><title>Journal of Geophysical Research. B. Solid Earth</title><addtitle>J. Geophys. Res</addtitle><description>Distinctive cloud trails are identified in Mars Reconnaissance Orbiter Mars Color Imager (MARCI) images over specific locations associated with Valles Marineris and Noctis Labyrinthus and at perihelion solar longitudes (LS = 230°–260°). High‐contrast surface shadows are well defined, as cast from their eastern margins, supporting altitude and optical depth determinations. These relatively high altitude clouds (40–50 km) exhibit narrow latitudinal widths (25–75 km) in comparison to extended longitudinal dimensions (400–1000 km). MARCI multispectral imaging of cloud surface shadows in five wavelength channels (260, 320, 437, 546, and 653 nm) yields the wavelength dependence of cloud extinction optical depth, revealing a range of small cloud particle sizes (reff = 0.2–0.5 μm) and moderate cloud optical depths (0.03–0.10 visible and 0.1–0.2 ultraviolet). Local time and temporal sampling characteristics of MARCI cloud images indicate that these clouds develop very rapidly in afternoon hours (1300–1500 LT), reach their full longitudinal extents within <2 h time scales, and often reoccur on successive afternoons. Mars Global Surveyor Mars Orbital Camera imaging in previous Mars years indicates these clouds are annually repeating. These observed characteristics suggest a cloud formation mechanism that is specific to ∼50 km horizontal and vertical scales, transports water vapor and dust upward from lower levels, exists during the afternoon, and is likely associated with the mesoscale atmospheric circulations induced by the near‐equatorial canyons of Mars. Cloud particles formed in such updrafts would then be rapidly transported westward in the strong retrograde zonal circulation of the subsolar middle atmosphere in this season.</description><subject>Altitude</subject><subject>Atmosphere</subject><subject>Atmospheric sciences</subject><subject>Canyons</subject><subject>Chemistry</subject><subject>Clouds</subject><subject>Earth sciences</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Mars</subject><subject>Optical analysis</subject><subject>Physics</subject><subject>Planetology</subject><subject>Planets</subject><subject>Water vapor</subject><issn>0148-0227</issn><issn>2169-9097</issn><issn>2156-2202</issn><issn>2169-9100</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2009</creationdate><recordtype>article</recordtype><recordid>eNqF0EtLAzEUBeAgCpbanVuhCOrG0Zub5yxFalV8UV_LkM4kMDXt1KRF_fdOaRFxUbPJ5jsnuZeQXQonFDA_RQB93QNgDNkGaSEVMkME3CQtoFxngKi2SSelETSHC8mBtsjeiw3Bpe6tjdXExSp1i1DPy-4s2iqkHbLlbUius7rb5Pmi93R-md3c96_Oz26yQoDQmUVmuVNUeKtzjUBRuKEvvCxR-RK8c1b4MgcoS6oZZ7mXWCjFPC2Hcigla5OjZe801u9zl2ZmXKXChWAnrp4no7Rq3kHOGnm4VjLJUXDAfyFSpkDni8b9P3BUz-OkGddoSSkFpnSDjpeoiHVK0XkzjdXYxi9DwSzWb36vv-EHq06bCht8tJOiSj8ZRJRci4XDpfuogvta22mu-4MeSrb4S7YMVWnmPn9CNr4ZqZgS5vWub2DwqB6kRDNg38V2nfk</recordid><startdate>20091104</startdate><enddate>20091104</enddate><creator>Clancy, R. 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Todd ; Wolff, Michael J. ; Cantor, Bruce A. ; Malin, Michael C. ; Michaels, Timothy I.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c5058-a23a4e715fa89820125ebfcf6d27fd0feea5fd900dd183439f62c773f1db6b663</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2009</creationdate><topic>Altitude</topic><topic>Atmosphere</topic><topic>Atmospheric sciences</topic><topic>Canyons</topic><topic>Chemistry</topic><topic>Clouds</topic><topic>Earth sciences</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Mars</topic><topic>Optical analysis</topic><topic>Physics</topic><topic>Planetology</topic><topic>Planets</topic><topic>Water vapor</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Clancy, R. Todd</creatorcontrib><creatorcontrib>Wolff, Michael J.</creatorcontrib><creatorcontrib>Cantor, Bruce A.</creatorcontrib><creatorcontrib>Malin, Michael C.</creatorcontrib><creatorcontrib>Michaels, Timothy I.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>AUTh Library subscriptions: ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest Natural Science Collection</collection><collection>Earth, Atmospheric & Aquatic Science Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>ProQuest Science Journals</collection><collection>ProQuest advanced technologies & aerospace journals</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>Earth, Atmospheric & Aquatic Science Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><collection>ASFA: Aquatic Sciences and Fisheries Abstracts</collection><collection>Aquatic Science & Fisheries Abstracts (ASFA) 2: Ocean Technology, Policy & Non-Living Resources</collection><collection>Aquatic Science & Fisheries Abstracts (ASFA) Professional</collection><collection>Earthquake Engineering Abstracts</collection><collection>Engineering Research Database</collection><collection>Civil Engineering Abstracts</collection><jtitle>Journal of Geophysical Research. B. Solid Earth</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Clancy, R. Todd</au><au>Wolff, Michael J.</au><au>Cantor, Bruce A.</au><au>Malin, Michael C.</au><au>Michaels, Timothy I.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Valles Marineris cloud trails</atitle><jtitle>Journal of Geophysical Research. B. Solid Earth</jtitle><addtitle>J. Geophys. Res</addtitle><date>2009-11-04</date><risdate>2009</risdate><volume>114</volume><issue>E11</issue><epage>n/a</epage><issn>0148-0227</issn><issn>2169-9097</issn><eissn>2156-2202</eissn><eissn>2169-9100</eissn><abstract>Distinctive cloud trails are identified in Mars Reconnaissance Orbiter Mars Color Imager (MARCI) images over specific locations associated with Valles Marineris and Noctis Labyrinthus and at perihelion solar longitudes (LS = 230°–260°). High‐contrast surface shadows are well defined, as cast from their eastern margins, supporting altitude and optical depth determinations. These relatively high altitude clouds (40–50 km) exhibit narrow latitudinal widths (25–75 km) in comparison to extended longitudinal dimensions (400–1000 km). MARCI multispectral imaging of cloud surface shadows in five wavelength channels (260, 320, 437, 546, and 653 nm) yields the wavelength dependence of cloud extinction optical depth, revealing a range of small cloud particle sizes (reff = 0.2–0.5 μm) and moderate cloud optical depths (0.03–0.10 visible and 0.1–0.2 ultraviolet). Local time and temporal sampling characteristics of MARCI cloud images indicate that these clouds develop very rapidly in afternoon hours (1300–1500 LT), reach their full longitudinal extents within <2 h time scales, and often reoccur on successive afternoons. Mars Global Surveyor Mars Orbital Camera imaging in previous Mars years indicates these clouds are annually repeating. These observed characteristics suggest a cloud formation mechanism that is specific to ∼50 km horizontal and vertical scales, transports water vapor and dust upward from lower levels, exists during the afternoon, and is likely associated with the mesoscale atmospheric circulations induced by the near‐equatorial canyons of Mars. Cloud particles formed in such updrafts would then be rapidly transported westward in the strong retrograde zonal circulation of the subsolar middle atmosphere in this season.</abstract><cop>Washington, DC</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2008JE003323</doi><tpages>9</tpages><oa>free_for_read</oa></addata></record> |
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subjects | Altitude Atmosphere Atmospheric sciences Canyons Chemistry Clouds Earth sciences Earth, ocean, space Exact sciences and technology Mars Optical analysis Physics Planetology Planets Water vapor |
title | Valles Marineris cloud trails |
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